# Constraint on the maximum mass of neutron stars using GW170817 event

@article{Shibata2019ConstraintOT,
title={Constraint on the maximum mass of neutron stars using GW170817 event},
author={Masaru Shibata and E.-P. Zhou and Kenta Kiuchi and Sho Fujibayashi},
journal={Physical Review D},
year={2019}
}
We revisit the constraint on the maximum mass of cold spherical neutron stars coming from the observational results of GW170817. We develop a new framework for the analysis by employing both energy and angular momentum conservation laws as well as solid results of latest numerical-relativity simulations and of neutron stars in equilibrium. The new analysis shows that the maximum mass of cold spherical neutron stars can be only weakly constrained as $M_{\rm max} \alt 2.3M_\odot$. Our present…

## Figures and Tables from this paper

Spin-polarized Neutron Matter, the Maximum Mass of Neutron Stars, and GW170817
• Physics
• 2019
We investigate how a phase transition from neutron-star matter to spin-polarized neutron matter affects the equation of state and mass-radius relation of neutron stars. While general extension
Delta baryons and diquark formation in the cores of neutron stars
• Physics
• 2020
We investigate the hadron-quark phase transition in cold neutron stars in light of (i) the observed limits on the maximum-mass of heavy pulsars, (ii) constraints on the tidal properties inferred from
Birth events, masses and the maximum mass of Compact Stars
• Physics
• 2020
We give in this Chapter an overview of the problem of neutron star mass distribution, the issue of the maximum mass as inferred from the existing sample and the new gravitational wave events, and the
Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints
What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?
• Physics
• 2019
The post-merger product of the first binary neutron star merger event detected in gravitational waves, GW170817, depends on neutron star equation of state (EoS) and is not well determined. We
Astrophysical Aspects of General Relativistic Mass Twin Stars
• Physics
• 2019
In this chapter we will introduce an effective equation of state (EoS) model based on polytropes that serves to study the so called "mass twins" scenario, where two compact stars have approximately
What can neutron stars reveal about the equation of state of dense matter?
Neutron stars are astrophysical objects of extremes, reaching the highest densities we can observe in the cosmos, and probing matter under conditions that cannot be recreated in terrestrial
Role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a neutron star with unified equations of state
• Physics
Physical Review C
• 2019
The role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a cold nonaccreted neutron star is studied using a set of unified equations of state. Based on the
Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant
GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts,
Maximum mass cutoff in the neutron star mass distribution and the prospect of forming supramassive objects in the double neutron star mergers
• Physics
• 2020
The sample of neutron stars with a measured mass is growing quickly. With the latest sample, we adopt both a flexible Gaussian mixture model and a Gaussian plus Cauchy-Lorentz component model to

## References

SHOWING 1-10 OF 79 REFERENCES
Gravitational-Wave Luminosity of Binary Neutron Stars Mergers.
• Physics, Medicine
Physical review letters
• 2018
The gravitational-wave luminosity and radiated energy of quasicircular neutron star mergers are studied using a large sample of numerical relativity simulations and it is found that there is an empirical universal relation connecting the total gravitational radiation and the angular momentum of the remnant.
Radiation of Angular Momentum by Neutrinos from Merged Binary Neutron Stars
• Physics
• 1998
We study neutrino emission from the remnant of an inspiraling binary neutron star following coalescence. The mass of the merged remnant is likely to exceed the stability limit of a cold, rotating
Gravitational waves and neutrino emission from the merger of binary neutron stars.
• Physics, Medicine
Physical review letters
• 2011
The neutrino luminosity curve when a black hole is formed for the first time is presented and the effective amplitude of gravitational waves from the HMNS is 4-6×10(-22) at f=2.1-2.5  kHz.
Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817.
• Physics, Medicine
Physical review letters
• 2018
The results are the first measurement of tidal deformability with a physical constraint on the star's equation of state and place the first lower bounds on the deformability and areal radii of neutron stars using gravitational waves.
GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass.
• Physics, Medicine
Physical review. D.
• 2018
Recent numerical simulations in general relativistic magnetohydrodynamics (GRMHD) provide useful constraints for the interpretation of the GW170817 discovery, leading to a bound on the maximum mass of a cold, spherical neutron star (the TOV limit): Mmaxsph≲2.74/β.
A two-solar-mass neutron star measured using Shapiro delay
• Physics, Medicine
Nature
• 2010
Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.
GW170817: Measurements of Neutron Star Radii and Equation of State.
This analysis expands upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars.
Remnant massive neutron stars of binary neutron star mergers: Evolution process and gravitational waveform
Massive (hypermassive and supramassive) neutron stars are likely to be often formed after the merger of binary neutron stars. We explore the evolution process of the remnant massive neutron stars and
The Influence of Thermal Pressure on Equilibrium Models of Hypermassive Neutron Star Merger Remnants
The merger of two neutron stars leaves behind a rapidly spinning hypermassive object whose survival is believed to depend on the maximum mass supported by the nuclear equation of state (EOS), angular
Gravitational waves from remnant massive neutron stars of binary neutron star merger: Viscous hydrodynamics effects
• Physics
• 2017
Employing a simplified version of the Israel-Stewart formalism of general-relativistic shear-viscous hydrodynamics, we explore the evolution of a remnant massive neutron star of binary neutron star